Title: Core collapse supernova gravitational wave emission for progenitors of 9.6, 15, and 25 M ⊙

Abstract

Here, we present gravitational wave emission predictions based on three core collapse supernova simulations corresponding to three different progenitor masses. The masses span a large range, between 9.6 and 25M_⊙, are all initially nonrotating, and are of two metallicities: zero and solar. We compute both the temporal evolution of the gravitational wave strains for both the plus and the cross polarizations, as well as their spectral decomposition and characteristic strains. The temporal evolution of our zero metallicity 9.6M_⊙ progenitor model is distinct from the temporal evolution of our solar metallicity 15M_⊙ progenitor model and our zero metallicity 25M_⊙ progenitor model. In the former case, the high-frequency gravitational wave emission is largely confined to a brief time period ~75 ms after bounce, whereas in the latter two cases high-frequency emission does not commence until ~125 ms after bounce or later. The excitation mechanisms of the high-frequency emission in all three cases correspond to proto-neutron star convection and accretion onto the proto-neutron star from the convective gain layer above it, with the former playing the dominant role for most of the evolution. The low-frequency emission in all three models exhibits very similar behavior. At frequencies below ~250 Hz, gravitational waves are emittedmore » by neutrino-driven convection and the standing accretion shock instability (SASI). This emission extends throughout the simulations when a gain region is present. In all three models, explosion is observed at ~125, ~500, and ~250 ms after bounce in the 9.6, 15, and 25M_⊙ progenitor models, respectively. At these times, the low-frequency gravitational wave emission is joined by very low-frequency emission, below ~10 Hz. These very low-frequency episodes are the result of explosion and begin at the above designated explosion times in each of our models. Our characteristic strains tell us that, in principle, all three gravitational wave signals would be detectable by current-generation detectors for a supernova at a distance of 10 kpc. However, our 9.6M_⊙ progenitor model is a significantly weaker source of gravitational waves, with strain amplitudes approximately 5–10 times less than in our other two models. The characteristic strain for this model tells us that such a supernova would be detectable only within a much more narrow frequency range around the maximum sensitivity of today’s detectors. Finally, in our 9.6M_⊙ progenitor model, we see very high-frequency gravitational radiation, extending up to ~2000 Hz. This feature results from the interaction of shock- and deleptonization-induced convection with perturbations introduced in the progenitor by nuclear burning during core collapse. While unique to the 9.6M_⊙ progenitor model analyzed here, this very high-frequency emission may, in fact, be a generic feature of the predictions for the gravitational wave emission from all core collapse supernova models when simulations are performed with three-dimensional progenitors.« less

Authors:

Mezzacappa, Anthony  ^[1];

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Marronetti, Pedro  ^[2];

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• Search DOE PAGES for ORCID "0000-0003-3070-0625"

Landfield, Ryan E.  ^[3];

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Lentz, Eric J.  ^[4];

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Murphy, R. Daniel ^[1]; Raphael Hix, W.  ^[5];

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• Search DOE PAGES for ORCID "0000-0002-9481-9126"

Harris, J. Austin  ^[3];

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Bruenn, Stephen W.  ^[6];

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Blondin, John M.  ^[7];

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Messer, II, O. E.  Bronson  ^[8];

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Casanova, Jordi  ^[9];

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• Search DOE PAGES for ORCID "0000-0002-9662-9588"

Kronzer, Luke L.  ^[10]

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• Search DOE PAGES for ORCID "0000-0001-5895-9255"

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+ Show Author Affiliations

1. Univ. of Tennessee, Knoxville, TN (United States)
2. National Science Foundation (NSF), Alexandria, VA (United States)
3. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). National Center for Computational Sciences (NCCS)
4. Univ. of Tennessee, Knoxville, TN (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division; Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Joint Institute for Nuclear Physics and its Applications
5. Univ. of Tennessee, Knoxville, TN (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division
6. Florida Atlantic Univ., Boca Raton, FL (United States)
7. North Carolina State Univ., Raleigh, NC (United States)
8. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). National Center for Computational Sciences (NCCS); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division
9. Community College of Denver, CO (United States)
10. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division; Univ. of Alabama, Tuscaloosa, AL (United States)

Publication Date:

Thu Feb 09 00:00:00 EST 2023

Research Org.:

Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)

Sponsoring Org.:

USDOE Office of Science (SC), Nuclear Physics (NP); National Science Foundation (NSF)

OSTI Identifier:

1928942

Grant/Contract Number:  

AC05-00OR22725; AC02-06CH11357; 1806692; 2110177

Resource Type:

Accepted Manuscript

Journal Name:

Physical Review. D.

Additional Journal Information:

Journal Volume: 107; Journal Issue: 4; Journal ID: ISSN 2470-0010

Publisher:

American Physical Society (APS)

Country of Publication:

United States

Language:

English

Subject:

79 ASTRONOMY AND ASTROPHYSICS; gravitation; gravitational waves; novae & supernovae; transient & explosive astronomical phenomena